Interaction of Particles with Matter

Interaction of Particles with Matter Werner Riegler, CERN, werner.riegler@cern.ch Danube School on Instrumentation in Elementary Particle & Nuclear Physics University of Novi Sad, Serbia, September 8th-13th, 2014. 1

On Tools and Instrumentation New directions in science are launched by new tools much more often than by new concepts. The effect of a concept-driven revolution is to explain old things in new ways. The effect of a tool-driven revolution is to discover new things that have to be explained Freeman Dyson, Imagined Worlds New tools and technologies will be extremely important to go beyond LHC 2

Physics Nobel Prices for Instrumentation 1927: C.T.R. Wilson, Cloud Chamber 1939: E. O. Lawrence, Cyclotron & Discoveries 1948: P.M.S. Blacket, Cloud Chamber & Discoveries 1950: C. Powell, Photographic Method & Discoveries 1954: Walter Bothe, Coincidence method & Discoveries 1960: Donald Glaser, Bubble Chamber 1968: L. Alvarez, Hydrogen Bubble Chamber & Discoveries 1992: Georges Charpak, Multi Wire Proportional Chamber All Nobel Price Winners related to the Standard Model: 87! (personal statistics by W. Riegler) 31 for Standard Model Experiments 13 for Standard Model Instrumentation and Experiments 3 for Standard Model Instrumentation 21 for Standard Model Theory 9 for Quantum Mechanics Theory 9 for Quantum Mechanics Experiments 1 for Relativity 56 for Experiments and instrumentation 31 for Theory 3

The Real World of Particles E. Wigner: A particle is an irreducible representation of the inhomogeneous Lorentz group Spin=0,1/2,1,3/2 Mass>0 E.g. in Steven Weinberg, The Quantum Theory of Fields, Vol1

The Real World of Particles W. Riegler: a particle is an object that interacts with your detector such that you can follow it s track, it interacts also in your readout electronics and will break it after some time, and if you a silly enough to stand in an intense particle beam for some time you will be dead

Particle Detector Systems 6

Cloud Chamber Wilson Cloud Chamber 1911 7

Cloud Chamber X-rays, Wilson 1912 Alphas, Philipp 1926 8

Cloud Chamber Magnetic field 15000 Gauss, chamber diameter 15cm. A 63 MeV positron passes through a 6mm lead plate, leaving the plate with energy 23MeV. The ionization of the particle, and its behaviour in passing through the foil are the same as those of an electron. Positron discovery, Carl Andersen 1933 9

Cloud Chamber Particle momenta are measured by the bending in the magnetic field. The V0 particle originates in a nuclear Interaction outside the chamber and decays after traversing about one third of the chamber. The momenta of the secondary particles are 1.6+-0.3 BeV/c and the angle between them is 12 degrees By looking at the specific ionization one can try to identify the particles and by assuming a two body decay on can find the mass of the V0. if the negative particle is a negative proton, the mass of the V0 particle is 2200 m, if it is a Pi or Mu Meson the V0 particle mass becomes about 1000m Rochester and Wilson 10

Nuclear Emulsion Film played an important role in the discovery of radioactivity but was first seen as a means of studying radioactivity rather than photographing individual particles. Between 1923 and 1938 Marietta Blau pioneered the nuclear emulsion technique. E.g. Emulsions were exposed to cosmic rays at high altitude for a long time (months) and then analyzed under the microscope. In 1937, nuclear disintegrations from cosmic rays were observed in emulsions. The high density of film compared to the cloud chamber gas made it easier to see energy loss and disintegrations. 11

Nuclear Emulsion Discovery of the Pion: The muon was discovered in the 1930ies and was first believed to be Yukawa s meson that mediates the strong force. The long range of the muon was however causing contradictions with this hypothesis. In 1947, Powell et. al. discovered the Pion in Nuclear emulsions exposed to cosmic rays, and they showed that it decays to a muon and an unseen partner. Discovery of muon and pion The constant range of the decay muon indicated a two body decay of the pion. 12

Bubble Chamber In the early 1950ies Donald Glaser tried to build on the cloud chamber analogy: Instead of supersaturating a gas with a vapor one would superheat a liquid. A particle depositing energy along it s path would then make the liquid boil and form bubbles along the track. In 1952 Glaser photographed first Bubble chamber tracks. Luis Alvarez was one of the main proponents of the bubble chamber. The size of the chambers grew quickly 1954: 2.5 (6.4cm) 1954: 4 (10cm) 1956: 10 (25cm) 1959: 72 (183cm) 1963: 80 (203cm) 1973: 370cm 13

Bubble Chamber old bubbles new bubbles Unlike the Cloud Chamber, the Bubble Chamber could not be triggered, i.e. the bubble chamber had to be already in the superheated state when the particle was entering. It was therefore not useful for Cosmic Ray Physics, but as in the 50ies particle physics moved to accelerators it was possible to synchronize the chamber compression with the arrival of the beam. For data analysis one had to look through millions of pictures. 14

Bubble Chamber BNL, First Pictures 1963, 0.03s cycle Discovery of the Ω - in 1964 15

Geiger Rutherford In 1908, Rutherford and Geiger developed an electric device to measure alpha particles. Rutherford and Geiger 1908 The alpha particles ionize the gas, the electrons drift to the wire in the electric field and they multiply there, causing a large discharge which can be measured by an electroscope. The random discharges in absence of alphas were interpreted as instability, so the device wasn t used much. Tip counter, Geiger 1913 As an alternative, Geiger developed the tip counter, that became standard for radioactive experiments for a number of years. 16

Detector + Electronics 1929 In 1928 Walther Müller started to study the sponteneous discharges systematically and found that they were actually caused by cosmic rays discovered by Victor Hess in 1911. Zur Vereinfachung von Koinzidenzzählungen W. Bothe, November 1929 Coincidence circuit for 2 tubes By realizing that the wild discharges were not a problem of the counter, but were caused by cosmic rays, the Geiger-Müller counter went, without altering a single screw from a device with fundametal limits to the most sensitive intrument for cosmic rays physics. 17

1930-1934 Cosmic ray telescope 1934 Rossi 1930: Coincidence circuit for n tubes 18

Scintillators, Cerenkov light, Photomultipliers In the late 1940ies, scintillation counters and Cerenkov counters exploded into use. Scintillation of materials on passage of particles was long known. By mid 1930 the bluish glow that accompanied the passage of radioactive particles through liquids was analyzed and largely explained (Cerenkov Radiation). Mainly the electronics revolution begun during the war initiated this development. High-gain photomultiplier tubes, amplifiers, scalers, pulse-height analyzers. 19

Anti Neutrino Discovery 1959 ν + p n + e + Reines and Cowan experiment principle consisted in using a target made of around 400 liters of a mixture of water and cadmium chloride. The anti-neutrino coming from the nuclear reactor interacts with a proton of the target matter, giving a positron and a neutron. The positron annihilates with an electron of the surrounding material, giving two simultaneous photons and the neutron slows down until it is eventually captured by a cadmium nucleus, implying the emission of photons some 15 microseconds after those of the positron annihilation. 20

Multi Wire Proportional Chamber Tube, Geiger- Müller, 1928 Multi Wire Geometry, in H. Friedmann 1949 G. Charpak 1968, Multi Wire Proportional Chamber, readout of individual wires and proportional mode working point. 21

MWPC Individual wire readout: A charged particle traversing the detector leaves a trail of electrons and ions. The wires are on positive HV. The electrons drift to the wires in the electric field and start to form an avalanche in the high electric field close to the wire. This induces a signal on the wire which can be read out by an amplifier. Measuring this drift time, i.e. the time between passage of the particle and the arrival time of the electrons at the wires, made this detector a precision positioning device. 22

W, Z-Discovery 1983/84 UA1 used a very large wire chamber. Can now be seen in the CERN Microcosm Exhibition This computer reconstruction shows the tracks of charged particles from the proton-antiproton collision. The two white tracks reveal the Z's decay. They are the tracks of a highenergy electron and positron. 23

LEP 1988-2000 All Gas Detectors 24

LEP 1988-2000 Aleph Higgs Candidate Event: e + e - HZ bb + jj 25

9/9/2014 Increasing Multiplicities in Heavy Ion Collisions e+ e- collision in the ALEPH Experiment/LEP. Au+ Au+ collision in the STAR Experiment/RHIC Up to 2000 tracks Pb+ Pb+ collision in the ALICE Experiment/LHC Up to 10 000 tracks/collision 26 W. Riegler

ATLAS at LHC Large Hadron Collider at CERN. 27 The ATLAS detector uses more than 100 million detector channels.

AMANDA Antarctic Muon And Neutrino Detector Array 28

AMANDA South Pole 29

AMANDA Photomultipliers in the Ice, looking downwards. Ice is the detecting medium. 30

AMANDA Look for upwards going Muons from Neutrino Interactions. Cherekov Light propagating through the ice. Find neutrino point sources in the universe! 31

Event Display AMANDA The Ice Cube neutrino observatory is designed so that 5,160 optical sensors view a cubic kilometer of clear South Polar ice. Up to now: No significant point sources but just neutrinos from cosmic ray interactions in the atmosphere were found. 32

CERN Neutrino Gran Sasso (CNGS) 33

Tau Candidate seen! Hypothesis: t (parent) hadron (daughter) + p 0 (decaying instantly to g 1, g 2 )+ n t (invisible)

AMS Alpha Magnetic Spectrometer Try to find Antimatter in the primary cosmic rays. Study cosmic ray composition etc. etc. Was launched into space on STS-134 on 16 May 2011. 35

AMS AMS Installed on the space station. 36

AMS A state of the art particle detector with many earth bound techniques going to space! 37

AMS 38

Detector Physics Precise knowledge of the processes leading to signals in particle detectors is necessary. The detectors are nowadays working close to the limits of theoretically achievable measurement accuracy even in large systems. Due to available computing power, detectors can be simulated to within 5-10% of reality, based on the fundamental microphysics processes (atomic and nuclear crossections) e.g. GEANT, FLUKA, MAGBOTLZ, HEED, GARFIELD 39

Electric Fields in a Micromega Detector Particle Detector Simulation Very accurate simulations of particle detectors are possible due to availability of Finite Element simulation programs and computing power. Follow every single electron by applying first principle laws of physics. For Gaseous Detectors: GARFIELD by R. Veenhof Electric Fields in a Micromega Detector Electrons avalanche multiplication 40

Particle Detector Simulation I) C. Moore s Law: Computing power doubles 18 months. II) W. Riegler s Law: The use of brain for solving a problem is inversely proportional to the available computing power. I) + II) =... Knowing the basics of particle detectors is essential 41

Interaction of Particles with Matter Any device that is to detect a particle must interact with it in some way almost In many experiments neutrinos are measured by missing transverse momentum. E.g. e + e - collider. P tot =0, If the Σ p i of all collision products is 0 neutrino escaped. Claus Grupen, Particle Detectors, Cambridge University Press, Cambridge 1996 (455 pp. ISBN 0-521-55216-8) 42

Interaction of Particles with Matter 43

How can a particle detector distinguish the hundreds of particles that we know by now?

These are all the known 27 particles with a lifetime that is long enough such that at GeV energies they travel more than 1 micrometer.

The 8 Particles a Detector must be able to Measure and Identify

The 8 Particles a Detector must be able to Measure and Identify

Creation of the Signal 9/9/2014 51

Detectors based on Registration of Ionization: Tracking in Gas and Solid State Detectors Charged particles leave a trail of ionization (and excited atoms) along their path: Electron-Ion pairs in gases and liquids, electron hole pairs in solids. The produced charges can be registered Position measurement Tracking Detectors. Cloud Chamber: Charges create drops photography. Bubble Chamber: Charges create bubbles photography. Emulsion: Charges blacked the film. Gas and Solid State Detectors: Moving Charges (electric fields) induce electronic signals on metallic electrons that can be read by dedicated electronics. In solid state detectors the charge created by the incoming particle is sufficient. In gas detectors (e.g. wire chamber) the charges are internally multiplied in order to provide a measurable signal. Tracking Detectors 52

1/ The induced signals are readout out by dedicated electronics. The noise of an amplifier determines whether the signal can be registered. Signal/Noise >>1 The noise is characterized by the Equivalent Noise Charge (ENC) = Charge signal at the input that produced an output signal equal to the noise. ENC of very good amplifiers can be as low as 50e-, typical numbers are ~ 1000e-. I=2.9eV 2.5 x 10 6 e/h pairs/cm In order to register a signal, the registered charge must be q >> ENC i.e. typically q>>1000e-. Gas Detector: q=80e- /cm too small. Solid state detectors have 1000x more density and factor 5-10 less ionization energy. Primary charge is 10 4-10 5 times larger than is gases. Gas detectors need internal amplification in order to be sensitive to single particle tracks. ßγ Without internal amplification they can only be used for a large number of particles that arrive at the same time (ionization chamber). 53

Principle of Signal Induction by Moving Charges A point charge q at a distance z 0 Above a grounded metal plate induces a surface charge. The total induced charge on the surface is q. Different positions of the charge result in different charge distributions. The total induced charge stays q. q q -q The electric field of the charge must be calculated with the boundary condition that the potential φ=0 at z=0. For this specific geometry the method of images can be used. A point charge q at distance z 0 satisfies the boundary condition electric field. -q The resulting charge density is (x,y) = 0 E z (x,y) (x,y)dxdy = -q I=0 54

Principle of Signal Induction by Moving Charges If we segment the grounded metal plate and if we ground the individual strips the surface charge density doesn t change with respect to the continuous metal plate. q V The charge induced on the individual strips is now depending on the position z 0 of the charge. If the charge is moving there are currents flowing between the strips and ground. -q The movement of the charge induces a current. -q I 1 (t) I 2 (t) I 3 (t) I 4 (t) 55

Signal Theorems What are the charges induced by a moving charge on electrodes that are connected with arbitrary linear impedance elements? One first removes all the impedance elements, connects the electrodes to ground and calculates the currents induced by the moving charge on the grounded electrodes. The current induced on a grounded electrode by a charge q moving along a trajectory x(t) is calculated the following way (Ramo Theorem): One removes the charge q from the setup, puts the electrode to voltage V 0 while keeping all other electrodes grounded. This results in an electric field E n (x), the Weighting Field, in the volume between the electrodes, from which the current is calculated by These currents are then placed as ideal current sources on a circuit where the electrodes are shrunk to simple nodes and the mutual electrode capacitances are added between the nodes. These capacitances are calculated from the weighting fields by 56

More on signal theorems, readout electronics etc. can be found in this book 57

Electromagnetic Interaction of Particles with Matter Z 2 electrons, q=-e 0 M, q=z 1 e 0 Interaction with the atomic electrons. The incoming particle loses energy and the atoms are excited or ionized. Interaction with the atomic nucleus. The particle is deflected (scattered) causing multiple scattering of the particle in the material. During this scattering a Bremsstrahlung photon can be emitted. In case the particle s velocity is larger than the velocity of light in the medium, the resulting EM shockwave manifests itself as Cherenkov Radiation. When the particle crosses the boundary between two media, there is a probability of the order of 1% to produced and X ray photon, called Transition radiation. 9/9/2014 W. Riegler, Particle Detectors 58

Ionization and Excitation F b x While the charged particle is passing another charged particle, the Coulomb Force is acting, resulting in momentum transfer The relativistic form of the transverse electric field doesn t change the momentum transfer. The transverse field is stronger, but the time of action is shorter The transferred energy is then The incoming particle transfer energy only (mostly) to the atomic electrons! 9/9/2014 W. Riegler, Particle Detectors 59

Ionization and Excitation Target material: mass A, Z 2, density [g/cm 3 ], Avogadro number N A A gramm N A Atoms: Number of atoms/cm 3 n a =N A /A [1/cm 3 ] Number of electrons/cm 3 n e =N A Z 2 /A [1/cm 3 ] With E(b) db/b = -1/2 de/e E max = E(b min ) E min = E(b max ) E min I (Ionization Energy) 9/9/2014 W. Riegler, Particle Detectors 60

Relativistic Collision Kinematics, E max θ φ 1) 2) 1+2) 9/9/2014 W. Riegler, Particle Detectors 61

Classical Scattering on Free Electrons 1/ This formula is up to a factor 2 and the density effect identical to the precise QM derivation Bethe Bloch Formula Electron Spin Density effect. Medium is polarized Which reduces the log. rise. 62

Bethe Bloch Formula 1/ Für Z>1, I 16Z 0.9 ev For Large g the medium is being polarized by the strong transverse fields, which reduces the rise of the energy loss density effect At large Energy Transfers (delta electrons) the liberated electrons can leave the material. In reality, E max must be replaced by E cut and the energy loss reaches a plateau (Fermi plateau). Characteristics of the energy loss as a function of the particle velocity ( g ) The specific Energy Loss 1/ρ de/dx first decreases as 1/ 2 increases with ln g for =1 is independent of M (M>>m e ) is proportional to Z 1 2 of the incoming particle. is independent of the material (Z/A const) shows a plateau at large g (>>100) de/dx 1-2 x ρ [g/cm 3 ] MeV/cm Energy Loss by Excitation and Ionization 63

Small energy loss Fast Particle Cosmis rays: de/dx α Z 2 Small energy loss Fast particle Pion Large energy loss Slow particle Discovery of muon and pion Pion Pion Kaon 64

Bethe Bloch Formula 1/ Bethe Bloch Formula, a few Numbers: For Z 0.5 A 1/ de/dx 1.4 MeV cm 2 /g for ßγ 3 Example : Iron: Thickness = 100 cm; ρ = 7.87 g/cm 3 de 1.4 * 100* 7.87 = 1102 MeV A 1 GeV Muon can traverse 1m of Iron This number must be multiplied with ρ [g/cm 3 ] of the Material de/dx [MeV/cm] Energy Loss by Excitation and Ionization 65

Energy Loss as a Function of the Momentum Energy loss depends on the particle velocity and is independent of the particle s mass M. The energy loss as a function of particle Momentum P= Mcβγ IS however depending on the particle s mass By measuring the particle momentum (deflection in the magnetic field) and measurement of the energy loss on can measure the particle mass Particle Identification! Energy Loss by Excitation and Ionization 66

Energy Loss as a Function of the Momentum Measure momentum by curvature of the particle track. Find de/dx by measuring the deposited charge along the track. Particle ID 67

Range of Particles in Matter Particle of mass M and kinetic Energy E 0 enters matter and looses energy until it comes to rest at distance R. Independent of the material Bragg Peak: For g>3 the energy loss is constant (Fermi Plateau) If the energy of the particle falls below g=3 the energy loss rises as 1/ 2 Towards the end of the track the energy loss is largest Cancer Therapy. Energy Loss by Excitation and Ionization 68

Relative Dose (%) Range of Particles in Matter Average Range: Towards the end of the track the energy loss is largest Bragg Peak Cancer Therapy Photons 25MeV Carbon Ions 330MeV Depth of Water (cm) Energy Loss by Excitation and Ionization 69

Luis Alvarez used the attenuation of muons to look for chambers in the Second Giza Pyramid Muon Tomography He proved that there are no chambers present. 9/9/2014 W. Riegler, Particle 70

Intermezzo: Crossection Crossection : Material with Atomic Mass A and density contains n Atoms/cm 3 E.g. Atom (Sphere) with Radius R: Atomic Crossection = R 2 p A volume with surface F and thickness dx contains N=nFdx Atoms. The total surface of atoms in this volume is N. The relative area is p = N /F = N A /A dx = Probability that an incoming particle hits an atom in dx. F dx What is the probability P that a particle hits an atom between distance x and x+dx? P = probability that the particle does NOT hit an atom in the m=x/dx material layers and that the particle DOES hit an atom in the m th layer Mean free path Average number of collisions/cm 9/9/2014 71

Intermezzo: Differential Crossection Differential Crossection: Crossection for an incoming particle of energy E to lose an energy between E and E +de Total Crossection: Probability P(E) that an incoming particle of Energy E loses an energy between E and E +de in a collision: Average number of collisions/cm causing an energy loss between E and E +de Average energy loss/cm: 9/9/2014 W. Riegler, Particle 72

Fluctuation of Energy Loss Up to now we have calculated the average energy loss. The energy loss is however a statistical process and will therefore fluctuate from event to event. x=0 x=d E X X X X X E - XX X X X X XXX X X XX X XXX X P( ) =? Probability that a particle loses an energy when traversing a material of thickness D We have see earlier that the probability of an interaction ocuring between distance x and x+dx is exponentially distributed

Probability for n Interactions in D We first calculate the probability to find n interactions in D, knowing that the probability to find a distance x between two interactions is P(x)dx = 1/ exp(-x/ ) dx with = A/ N A

Probability for n Interactions in D For an interaction with a mean free path of, the probability for n interactions on a distance D is given by Poisson Distribution! If the distance between interactions is exponentially distributed with an mean free path of λ the number of interactions on a distance D is Poisson distributed with an average of n=d/λ. How do we find the energy loss distribution? If f(e) is the probability to lose the energy E in an interaction, the probability p(e) to lose an energy E over the distance D?

d (E,E )/de / (E) Fluctuations of the Energy Loss Probability f(e) for loosing energy between E and E +de in a single interaction is given by the differential crossection d (E,E )/de / (E) which is given by the Rutherford crossection at large energy transfers Excitation and ionization Scattering on free electrons P(E, ) Energy Loss by Excitation and Ionization 76

Landau Distribution Landau Distribution P( ): Probability for energy loss in matter of thickness D. Landau distribution is very asymmetric. Average and most probable energy loss must be distinguished! Measured Energy Loss is usually smaller that the real energy loss: 3 GeV Pion: E max = 450MeV A 450 MeV Electron usually leaves the detector. Energy Loss by Excitation and Ionization 77

Landau Distribution LANDAU DISTRIBUTION OF ENERGY LOSS: PARTICLE IDENTIFICATION Requires statistical analysis of hundreds of samples Counts 4 cm Ar-CH4 (95-5) 6000 5 bars N = 460 i.p. Counts 6000 protons electrons 15 GeV/c 4000 FWHM~250 i.p. 4000 2000 2000 0 0 500 1000 For a Gaussian distribution: N (i.p.) N ~ 21 i.p. FWHM ~ 50 i.p. 0 0 500 1000 N (i.p) I. Lehraus et al, Phys. Scripta 23(1981)727 Energy Loss by Excitation and Ionization 78

Particle Identification Measured energy loss average energy loss In certain momentum ranges, particles can be identified by measuring the energy loss. Energy Loss by Excitation and Ionization 79

Bremsstrahlung A charged particle of mass M and charge q=z 1 e is deflected by a nucleus of charge Ze which is partially shielded by the electrons. During this deflection the charge is accelerated and it therefore radiated Bremsstrahlung. Z 2 electrons, q=-e 0 M, q=z 1 e 0 9/9/2014 W. Riegler, Particle 80

Bremsstrahlung, Classical A charged particle of mass M and charge q=z 1 e is deflected by a nucleus of Charge Ze. Because of the acceleration the particle radiated EM waves energy loss. Coulomb-Scattering (Rutherford Scattering) describes the deflection of the particle. Maxwell s Equations describe the radiated energy for a given momentum transfer. de/dx 81

Bremsstrahlung, QM Proportional to Z 2 /A of the Material. Proportional to Z 14 of the incoming particle. Proportional to of the material. Proportional 1/M 2 of the incoming particle. Proportional to the Energy of the Incoming particle E(x)=Exp(-x/X 0 ) Radiation Length X 0 M 2 A/ ( Z 14 Z 2 ) X 0 : Distance where the Energy E 0 of the incoming particle decreases E 0 Exp(-1)=0.37E 0. 82

Critical Energy For the muon, the second lightest particle after the electron, the critical energy is at 400GeV. The EM Bremsstrahlung is therefore only relevant for electrons at energies of past and present detectors. Electron Momentum 5 50 500 MeV/c Critical Energy: If de/dx (Ionization) = de/dx (Bremsstrahlung) Myon in Copper: Electron in Copper: p 400GeV p 20MeV 83

Pair Production, QM For Eg>>m e c 2 =0.5MeV : = 9/7X 0 Average distance a high energy photon has to travel before it converts into an e + e - pair is equal to 9/7 of the distance that a high energy electron has to travel before reducing it s energy from E 0 to E 0 *Exp(-1) by photon radiation. 84

Bremsstrahlung + Pair Production EM Shower 85

Multiple Scattering Statistical (quite complex) analysis of multiple collisions gives: Probability that a particle is defected by an angle after travelling a distance x in the material is given by a Gaussian distribution with sigma of: X 0... Radiation length of the material Z 1... Charge of the particle p... Momentum of the particle 86

Multiple Scattering Magnetic Spectrometer: A charged particle describes a circle in a magnetic field: Limit Multiple Scattering 87

Multiple Scattering 88

Multiple Scattering ATLAS Muon Spectrometer: N=3, sig=50um, P=1TeV, L=5m, B=0.4T p/p ~ 8% for the most energetic muons at LHC 89

Cherenkov Radiation If we describe the passage of a charged particle through material of dielectric permittivity (using Maxwell s equations) the differential energy crossection is >0 if the velocity of the particle is larger than the velocity of light in the medium is N is the number of Cherenkov Photons emitted per cm of material. The expression is in addition proportional to Z 12 of the incoming particle. The radiation is emitted at the characteristic angle c, that is related to the refractive index n and the particle velocity by M, q=z 1 e 0 90

Cherenkov Radiation 91

Ring Imaging Cherenkov Detector (RICH) There are only a few photons per event one needs highly sensitive photon detectors to measure the rings! 92

LHCb RICH 93

Transition Radiation Z 2 electrons, q=-e 0 M, q=z 1 e 0 When the particle crosses the boundary between two media, there is a probability of the order of 1% to produced and X ray photon, called Transition radiation. 9/9/2014 94

Transition Radiation 95

Electromagnetic Interaction of Particles with Matter Ionization and Excitation: Charged particles traversing material are exciting and ionizing the atoms. The average energy loss of the incoming particle by this process is to a good approximation described by the Bethe Bloch formula. The energy loss fluctuation is well approximated by the Landau distribution. Multiple Scattering and Bremsstrahlung: The incoming particles are scattering off the atomic nuclei which are partially shielded by the atomic electrons. Measuring the particle momentum by deflection of the particle trajectory in the magnetic field, this scattering imposes a lower limit on the momentum resolution of the spectrometer. The deflection of the particle on the nucleus results in an acceleration that causes emission of Bremsstrahlungs-Photons. These photons in turn produced e+e- pairs in the vicinity of the nucleus, which causes an EM cascade. This effect depends on the 2 nd power of the particle mass, so it is only relevant for electrons. 9/9/2014 96

Electromagnetic Interaction of Particles with Matter Cherenkov Radiation: If a particle propagates in a material with a velocity larger than the speed of light in this material, Cherenkov radiation is emitted at a characteristic angle that depends on the particle velocity and the refractive index of the material. Transition Radiation: If a charged particle is crossing the boundary between two materials of different dielectric permittivity, there is a certain probability for emission of an X-ray photon. The strong interaction of an incoming particle with matter is a process which is important for Hadron calorimetry and will be discussed later. 9/9/2014 97

Hadronic Calorimetry 98

Bremsstrahlung + Pair Production EM Shower λ λ λ λ Iron: X 0 =1.76cm λ=17cm 99

Conclusions Knowing the basic principles of interaction of particles with matter you can understand detector performance to 20% level on the back of an envelope. In addition it crucial knowledge when you think about a new instrumentation ideas. It is up to you to design the next generation of particle detectors!